The simulations are initialised with the asymmetric stellar wind of a blue
supergiant star. The adopted latitude-dependence of the wind density is that
developed in the context of the astrosphere of the runaway asymptotic giant
branch star Mira [1]}. It reads,
\(\rho _{w}(r,\theta ) = \frac{ \dot{M} }{ 4\pi r^{2} v_{\rm w} }\rightarrow \frac{ A }{ r^{2} }f( \theta ),\) 
